Adiabatic density perturbations and matter generation from the minimal supersymmetric standard model

Physical Review Letters

Volumn 90, Issue 9, 2003, Pages

  Enqvist, Kari ^a   Kasuya, Shinta ^a   Mazumdar, Anupam ^b  

^a UNIVERSITY OF HELSINKI   (Finland)

^b MCGILL UNIVERSITY   (Canada)

Author keywords

[No Author keywords available]

Indexed keywords

ASTROPHYSICS; CHARGED PARTICLES; GRAVITATION; MATHEMATICAL MODELS; OSCILLATIONS; PERTURBATION TECHNIQUES;

ADIABATIC DENSITY PERTURBATIONS; ENERGY DENSITY; MINIMAL SUPERSYMMETRIC STANDARD MODEL;

HIGH ENERGY PHYSICS;

EID: 0037424187     PISSN: 00319007     EISSN: None     Source Type: Journal    
DOI: None     Document Type: Article

References (34)

1. C. B. Netterfield et al., Astrophys. J. 571, 604 (2002).
2. A. T. Lee et al., Astrophys. J. 561, L1 (2001).
3. N. W. Halverson et al., Astrophys. J. 568, 38 (2002)
4. C. Pryke et al., Astrophys. J. 568, 46 (2002).
5. A. R. Liddle and D. H. Lyth, Cosmological Inflation and Large Scale Structure (Cambridge University Press, Cambridge, 2000).
6. T. Gherghetta, C. Kolda, and S. P. Martin, Nucl. Phys. B468, 37 (1996).
7. K. Enqvist and A. Mazumdar, hep-ph/0209244.
8. K. Enqvist and J. McDonald, Phys. Rev. Lett. 83, 2510 (1999).
9. K. Enqvist and J. McDonald, Phys. Rev. D 62, 043502 (2000).
10. M. Kawasaki and F. Takahashi, Phys. Lett. B 516, 388 (2001).
11. D. H. Lyth and D. Wands, Phys. Lett. B 524, 5 (2002).
12. K. Enqvist and M. S. Sloth, Nucl. Phys. B626, 395 (2002).
13. T. Moroi and T. Takahashi, Phys. Lett. B 522, 215 (2001)
14. Phys. Rev. D 66, 063501 (2002)
15. N. Bartolo and A. R. Liddle, Phys. Rev. D 65, 121301 (2002)
16. M. S. Sloth, hep-ph/0208241
17. D. H. Lyth, C. Ungarelli, and D. Wands, Phys. Rev. D 67, 023503 (2003)
18. K. Dimopoulos and D. H. Lyth, hep-ph/0209180
19. M. Bastero-Gil et al., hep-ph/0211011
20. T. Moroi and H. Murayama, hep-ph/0211019.
21. P. Binétruy and G. Dvali, Phys. Lett. B 388, 241 (1996).
22. M. K. Gaillard, H. Murayama, and K. A. Olive, Phys. Lett. B 355, 71 (1995).
23. M. Dine, L. Randall, and S. Thomas, Nucl. Phys. B458, 291 (1996).
24. Thermal corrections due to hidden radiation are negligible, since the flat direction couples to it only gravitationally. On the other hand, after the flat direction begins its oscillation, ordinary radiations is gradually produced by the decay of the flat direction, but its energy density is too small to affect the dynamics of the flat direction.
25. V. A. Rubakov and M. E. Shaposhnikov, Usp. Fiz. Nauk 166, 5 (1996) [Phys. Usp. 39, 461 (1996)].
26. G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rep. 267, 195 (1996).
27. K. Enqvist, A. Jokinen, S. Kasuya, and A. Mazumdar (to be published).
28. K. A. Olive, G. Steigman, and T. P. Walker, Phys. Rep. 333, 389 (2000).
29. For a nonminimal Kähler potential, it is possible to have some A terms. In this situation, it might be possible to have a right amount of the baryon asymmetry from the flat direction which acts as a curvaton [19].
30. Depending on the SUSY parameter values, the flat direction could first fragment to form Q balls.
31. J. Ellis, J. E. Kim, and D. V. Nanopoulos, Phys. Lett. B 145, 181 (1984)
32. A. L. Maroto and A. Mazumdar, Phys. Rev. Lett. 84, 1655 (2000)
33. R. Kallosh et al., Phys. Rev. D 61, 103503 (2000).
34. Gravitinos could, however, be produced thermally also by the hidden sector radiation. For low enough reheat temperature in the hidden sector, or for large enough entropy production due to the decay of the flat direction in the visible sector, there should be no gravitino problem [19].